where \(v_{Los}\)  is the line-of-sight velocity of the cluster in km/sec, \(\alpha \)  the distance from the cluster centre in the direction of motion in radians, \(D\)  the distance of the cluster from the Sun in kpc,
and \(A=4.74\)  [1]}, [2]}.
Using the above equation, VB21 determined moving group distances to about 40 globular clusters based on Gaia EDR3 proper motions and the average line-of-sight velocities of the clusters from
[3]}. Here we use the two most
precisely determined distances \(D=4.62 \pm 0.28\)  kpc (NGC 3201) and \(D=5.34 \pm 0.55\)  kpc (NGC 5139). For all other clusters the derived distances have too large error bars to be useful.
